Relativistic jets from XRBs with LOFAR. Stéphane Corbel (University Paris 7 & CEA Saclay)

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1 Relativistic jets from XRBs with LOFAR. Stéphane Corbel (University Paris 7 & CEA Saclay)

2 Outline Introduction: X-ray binaries and flavors of relativistic jets LOFAR Contributions Conclusions

3 Introduction: X-ray Binaries and flavors of relativistic jets LOFAR Contributions Conclusions

4 Introduction: X-ray binaries Image: R. Fender

5 X-ray States of Black Hole Binaries RXTE/ASM lightcurve of a typical X-ray nova Hardness of the X-ray spectra 1 Crab 1 years X Variable on many different timescales!! quiescence to outburst: days outburst : from s to days Radio properties : also very variable

6 Stirling et al Mirabel et al. 94 Two flavors of relativistic jets from microquasars: two very different scales!!!! Compact, self-absorbed jets (on mas scale = 10s a.u. ). Discrete ejections (superluminal, ballistic).

7 Spectral extent of these small scale jets Corbel et al. 05 Compact jet: flat spectrum, but self absorption in LOFAR frequency range Discrete ejections events: optically thin, but opacity delays for LOFAR Note: important connection with high energy properties

8 Jet unification Unification of jet properties: Hard state: compact jet Thermal state : no jet Transition hard IS to soft IS: Discrete and transient massive ejection event(s). (Corbel et al. 04, Fender et al. 04):

9 Large scale jets (or lobes) Dubner et al. 98 Mirabel et al. 92 Large scale lobes = long term action of impulsive relativistic events. Constant radio flux ISM = calorimeter See talk by C. Kaiser Gallo et al. 2005

Topics addressed Jet physics: Particles acceleration in accreting compact objects: shock acceleration, interaction with ISM, synchrotron radiation, explosive events, jet collimation.

10 Topics addressed Jet physics: Particles acceleration in accreting compact objects: shock acceleration, interaction with ISM, synchrotron radiation, explosive events, jet collimation. Jet energetics, Phase of energy loss that could be energy dependant ( sync or ic loss) or energy independent (adiabatic loss), all convolved with evolution of optical depth (important for LOFAR). Accretion ejection coupling. Impact of jets on ISM or IGM? Similarities XRB/AGN (ULX?)

11 Introduction: X-ray binaries and flavors of relativistic jets LOFAR Contributions Conclusions

12 Compact jets: flat radio spectrum Relativistic ejections and large scale lobes: radio spectrum rising in LOFAR freq range.

LOFAR as a Radio ASM Currently, any active X-ray sources is usually spotted by RXTE ASM (Movie) actual trigger for follow-up observations (space +ground). However likely no more ASM beyond 2008!

13 LOFAR as a Radio ASM Currently, any active X-ray sources is usually spotted by RXTE ASM (Movie) actual trigger for follow-up observations (space +ground). However likely no more ASM beyond 2008!! Major issue for transient sources such as XNe LOFAR = software telescope. Compact core can monitor large portion of the northern hemisphere sky + normal full-array to observe in more details any new transient

14 Reactivation of XRBs (Re)Activation of XRBs = hard state = compact jet. LOFAR = a much more sensitive ASM. E.g.: RXTE ASM 1 c/s ~ 1 mjy compact jet based on the radio/x-ray correlation that is observed in the associated hard X-ray state LOFAR RSM at 200 MHz has a 12 hr sensitivity of ~40 µjy (25x more sensitive than RXTE/ASM). + arcsec position can be delivered quickly Radio observations can now be the trigger for X-ray observations (contrary to the past!). Physics under extreme conditions (gravity, pressure, density) Serendipitous discoveries!!! Will there be any other ASM at the same time?

Synergy with the new forthcoming high energy observatory: GLAST Large Area Telescope (LAT) GLAST Burst Monitor (GBM) Large energy range: LAT (20 MeV-300 GeV).

15 Synergy with the new forthcoming high energy observatory: GLAST Large Area Telescope (LAT) GLAST Burst Monitor (GBM) Large energy range: LAT (20 MeV-300 GeV). GBM (10 kev 25 MeV) Huge FOV: LAT: 20% of the sky at any instant. All accessible sky observed 30 mn every 3 hr. Galactic Plane always visible every day. GBM: all accessible sky at any time Launch in December 2007

16 30 x more sensitive than previous similar experiment EGRET. 1 day with GLAST is ~similar to the lifetime of EGRET (9 years). Better PSF than EGRET better position (but at best 0.5 to 1 arcmin). Will need contribution from other facilities. Similar scientific objectives Probing the non-thermal universe (synchrotron vs. comptonization). LOFAR and GLAST together is an excellent opportunity!!!

18 Transient sources in the Galaxy Transient ejections: > GHz However, peak delayed at low freq + impact of expansion losses : peak ~ 5 times lower in LOFAR range + possibility of low freq self absorption (# from Fender s memo): Detection of initial event at 100s MHz will require the ability to detect a source as weak as 0.15 mjy (worst case for a BH). Feasible for the bright (> 0.5 Crab) transients (1 to 3 per year). No pb to get the peak flux few days later. Ability to detect the peak flux of fainter transients: 12 hr rms of ~ 40 µjy faint transients with peak flux of 10 mcrab. Up to 10 more sources.

19 Radio emission from a new bright transient will likely be detected at onset and for sure during the peak. Possibility to detect fainter transients: only detected several days after activation during the peak. Very rapid detection not possible (with exception if the event is initially opt thin). Pb of the buffer memory?? 1 to 15 transient to monitored by LOFAR Possibility to first detect radio transient in M31

20 Searching for microblazar Microquasar with a jet pointing towards the observer. One possible explanation for the nature of ULX? But not only, c.f. there should be some Galactic microblazars too! t α 1/2γ 2 and Ι α 8γ 3 : If γ = 5, Θ < 10 ο t < 1/50 and I > 10 3 : Fast and intense variation of radio flux density: need a RASM such as LOFAR. + Possibility of associated γ-ray inverse compton emission if intense external radiation field density (such as a massive donor star).

21 Scientific interest for low frequency radio obs Very rare observations in this range Simultaneous observations at low and high frequency of an ejection event: compare decay rates: radiative or expansion losses? Extent of the non-thermal electron spectrum: N(E)dE α E -p with p ~2: γ e ~ 5 GHz γ e ~ 150 MHz. Energetics dominated by kinetic energy of cold proton. Determination of minimum γ e Energy deposited in lobes (cf Cyg X-1): KE U in shock: steep spectrum : many new lobes Low freq abs processes (TR or free-free) : B + n e Unique capability to focus a posteriori to some specific event (GRB: prompt emission)

22 Conclusions LOFAR is a new unique opportunity: Radio all sky monitor. Synergy with forthcoming GLAST Compact jet sources Relativistic ejections Alerts for these explosive events Searching for microblazars Large scale jets see more in following talks

Stellar Binary Systems and CTA. Guillaume Dubus Laboratoire d Astrophysique de Grenoble

Stellar Binary Systems and CTA Guillaume Dubus Laboratoire d Astrophysique de Grenoble Barcelona Cherenkov Telescope Array Meeting, 24-25 January 2008 X-ray binaries picture by H. Spruit relativistic outflow